标题： 三维磁热模拟纠缠的中子星外壳磁场 显示英文标题

标题： 3D Magneto-thermal Simulations of Tangled Crustal Magnetic Field in Central Compact Objects

摘要： 中心致密天体是年轻的中子星，它们发出热X射线，其全波段光度$L_X$在$10^{32}$-$10^{34}$erg/s 的范围内。 Gourgouliatos、Hollerbach 和 Igoshev 最近提出，中心致密天体的特殊辐射特性可以通过在原中子星阶段由随机发电机形成的纠缠磁场配置来解释。 在这种情况下，磁场由多个小尺度成分组成，全球偶极场的贡献可以忽略不计。 我们数值研究了中子星中纠缠壳层磁场的三维磁热演化。 我们发现所有配置都会产生复杂的表面热图案，这些图案由多个小的热点组成，这些热点彼此之间有显著的距离。 初始磁场能量为$2.5-10\times 10^{47}$erg 的配置，热点温度可达$\approx 0.2$keV，与我们没有冷却模拟中的整体温度$\approx 0.1$keV 相比。 在中心致密天体的观测中也看到了温度相差两倍的情况。 热点会在光变曲线中产生周期性调制，典型振幅为$\leq 9-11$%。 因此，纠缠磁场配置可以解释一些中心致密天体的热辐射特性。 显示英文摘要

摘要： Central compact objects are young neutron stars emitting thermal X-rays with bolometric luminosities $L_X$ in the range $10^{32}$-$10^{34}$ erg/s. Gourgouliatos, Hollerbach and Igoshev recently suggested that peculiar emission properties of central compact objects can be explained by tangled magnetic field configurations formed in a stochastic dynamo during the proto-neutron star stage. In this case the magnetic field consists of multiple small-scale components with negligible contribution of global dipolar field. We study numerically three-dimensional magneto-thermal evolution of tangled crustal magnetic fields in neutron stars. We find that all configurations produce complicated surface thermal patterns which consist of multiple small hot regions located at significant separations from each other. The configurations with initial magnetic energy of $2.5-10\times 10^{47}$ erg have temperatures of hot regions that reach $\approx 0.2$ keV, to be compared with the bulk temperature of $\approx 0.1$ keV in our simulations with no cooling. A factor of two in temperature is also seen in observations of central compact objects. The hot spots produce periodic modulations in light curve with typical amplitudes of $\leq 9-11$ %. Therefore, the tangled magnetic field configuration can explain thermal emission properties of some central compact objects.